Black hole mass estimates from soft X-ray spectra

TL;DR

This paper discusses methods to estimate black hole masses from X-ray spectra, introduces a new accretion model, and suggests that certain ULXs can be explained by intermediate-mass black holes with specific accretion rates.

Contribution

It presents a new phenomenological model for high accretion states and provides insights into the spectral properties of ULXs and their possible black hole masses.

Findings

A standard disk dominates beyond a transition radius R_c.

Most accretion power inside R_c is released via non-thermal processes.

Black holes of 50-100 solar masses at high accretion rates can explain ULX spectra.

Abstract

In the absence of direct kinematic measurements, the mass of an accreting black hole is sometimes inferred from the X-ray spectral parameters of its accretion disk; specifically, from the temperature and normalization of a disk-blackbody model fit. Suitable corrections have to be introduced when the accretion rate approaches or exceeds the Eddington limit. We summarize phenomenological models that can explain the very high state, with apparently higher disk temperatures and lower inner-disk radii. Conversely, ultraluminous X-ray sources often contain cooler disks with large characteristic radii. We introduce another phenomenological model for this accretion state. We argue that a standard disk dominates the radiative output for radii larger than a characteristic transition radius R_c ~ mdot x R_{ISCO}, where mdot is the accretion rate in Eddington units and R_{ISCO} is the innermost stable orbit. For R_{ISCO} < R < R_c, most of the accretion power is released via non-thermal processes. We predict the location of such sources in a luminosity-temperature plot. We conclude that black holes with masses ~ 50-100 Msun accreting at mdot ~ 10-20 may explain the X-ray properties of many ULXs.